We determine a kinematic distance independently for each proper motion velocity dispersion profile that we have from either Gaia EDR3 or HST data. The best-fitting distance is determined by
fitting each cluster with the grid of \(N\) -body models calculated by [1]} and
[2]}. Their grid contains several thousand \(N\) -body models of star clusters, varying the size, initial density profile, metallicity
and stellar mass function of each cluster. We interpolate within this grid and determine for each cluster the \(N\) -body model that simultaneously provides the best fit to the internal mass function,
velocity dispersion and surface density profile. More details about the \(N\) -body models can be found in [1]} and
[2]} and we refer the reader to these papers for a full description of the fitting procedure.
